Implications of New JHK Photometry and a Deep Infrared Luminosity Function for the Galactic Bulge

We present deep near-IR photometry for Galactic bulge stars in Baade’s Window, $(l,b)=(1.0\mathrm{deg},-3.9\mathrm{deg}),$ and another minor axis field at $(l,b) = (0^\circ,-6^\circ)$. We combine our data with previously published photometry and construct a luminosity function over the range $5.5\le K_0\le 16.5$, deeper than any previously published. The slope of this luminosity function and the magnitude of the tip of the first ascent giant branch are consistent with theoretical values derived from isochrones with appropriate age and metallicity. We use the relationship between [Fe/H] and the giant branch slope derived from near-IR observations of metal rich globular clusters by Kuchinski {\it et al.} [AJ, 109, 1131 (1995)] to calculate the mean metallicity for several bulge fields along the minor axis. For Baade’s Window we derive $\langle {\rm[Fe/H]}\rangle = -0.28 \pm 0.16$, consistent with the recent estimate of McWilliam & Rich [ApJS, 91, 749 (1994)], but somewhat lower than previous estimates based on CO and TiO absorption bands and the $JHK$ colors of M giants by Frogel {\it et al.} [ApJ, 353, 494 (1990)]. Between $b=-3\mathrm{deg}$ and $-12\mathrm{deg}$ we find a gradient in $⟨[\mathrm{F}\mathrm{e}\mathrm{/}\mathrm{H}]⟩$ of $-0.06 \pm 0.03$dex\mathrm{/}degreeor$-0.43 \pm 0.21$dex\mathrm{/}kpcfor$R_0 = 8$ kpc, consistent with other independent derivations. We derive a helium abundance for Baade’s Window with the $R$ and $R^{\mathrm{\prime }}$ methods and find that $Y=0.27\pm 0.03$ implying $\mathrm{\Delta }Y\mathrm{/}\mathrm{\Delta }Z=3.3\pm 1.3$. Next, we find that the bolometric corrections for bulge K giants ($V - K \leq 2$) are in excellent agreement with empirical derivations based on observations of globular cluster and local field stars. However, for the redder M giants we